Iota Pegasi

From Wikipedia, the free encyclopedia
Jump to: navigation, search
Iota Pegasi
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Pegasus
Right ascension 22h 07m 00.666s[1]
Declination 25° 20′ 42.40″[1]
Apparent magnitude (V) 3.84/6.68[2]
Characteristics
Spectral type F5V/G9V
Astrometry
Proper motion (μ) RA: 296.53 ± 0.59[1] mas/yr
Dec.: 27.29 ± 0.58[1] mas/yr
Parallax (π) 85.28 ± 0.63[1] mas
Distance 38.2 ± 0.3 ly
(11.73 ± 0.09 pc)
Absolute magnitude (MV) 3.49/6.33[2]
Orbit
Companion Iota Pegasi B
Period (P) 0.028 yr
Semi-major axis (a) 0.0094"
Eccentricity (e) 0.02
Details
ι Peg A
Mass 1.33[2] M
Radius 1.526 ± 0.068[3] R
Surface gravity (log g) 4.26[2] cgs
Temperature 6,580[2] K
ι Peg B
Mass 0.82[2] M
Radius 0.73[2] R
Surface gravity (log g) 4.62[2] cgs
Temperature 5,060[2] K

Iota Pegasi (24 Peg, HD 210027) is a star located within the constellation Pegasus. It is about 38 light-years from Earth.[1] It is a spectroscopic binary system.[4]

Iota Pegasi A is a yellowish-white star somewhat brighter than the sun. It and the dimmer Iota Pegasi B orbit each other with a period of about 10 days. In about four billion years from now, component A will evolve off the main sequence into a giant. In the process it will overflow its Roche lobe and begin to transfer mass onto the secondary. This may cause the secondary to acquire enough mass to become the primary component. After both stars have passed through the giant star stage, the end result will be a pair of co-orbiting white dwarfs in about eight billion years.[2]

References[edit]

External links[edit]